The White Light Coronagraph aboard Spartan 201-03 spacecraft observed the
corona on 8, 9 and 10 of September 1995, at a height of 1.5-6.0 R_ødot fromSun center. In conjunction, the ground-based HAO K-coronameter (Mark-III)
observed the corona at a height of 1.15-2.1 R_ødot while the space-based
Soft X-ray Telescope (SXT) on Yohkoh observed the inner corona at a height of
0-1.5 R_ødot.

In this paper we explore the physical and
morphological characteristics of the large-scale coronal structures such as
polar coronal rays and high latitude streamers as seen in
white-light and
relate these structures to observations in soft X-ray (3-45 Åemissions to estimate their temperatures.
Past and persent analysis shows
that polar rays can be characterized by two temperature classes
depending upon the observed properties of the forbidden lines of FeX and FeXIV
and soft x-rays. Cool
rays are a dominant feature of the polar corona during the quiescent phase of
the solar cycle. The hot rays when present form a small subset of the array of
rays seen in white-light. Hot rays seem to emerge from the boundary of the polar coronal hole (polar
crown filament belt). The location of the cool rays on the other hand can be
anywhere inside the coronal hole.
We find the emission-line temperature to be high
(local maxima, 40-60% higher) in the high
latitude coronal streamers with enhanced white-light emission and associated
with new cycle high-latitude magnetic fields separated from the old cycle
polar field of opposite polarity.